The role of detailed gas and dust opacities in shaping the evolution of the inner disc edge subject to episodic accretion

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Volume 707 (March 2026)

A&A, 707 (2026) A296

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Table 2

Model names and configurations.

Model	Dust mean opacity [cm² g⁻¹ ]	Dust irradiation opacity [cm² g⁻¹]	Gas mean opacity [cm² g⁻¹]	Gas irradiation opacity [cm² g⁻¹]	Accretion luminosity
MREF^*	κ_P = κ_R = 700	κ_P = 1300	κ_P = κ_R = 10⁻³	κ_P = 10⁻³	no
DUST	$κ_{P, R}^{D I} (T_{g})$ $Mathematical equation: $\kappa_\mathrm{P,R}^\mathrm{DI}(T_\mathrm{g})$$	$κ^{D I} (ν)$ $Mathematical equation: $\kappa^\mathrm{DI}(\nu)$$	κ_P = κ_R = 10⁻³	κ_P = 10⁻³	yes/no
NOFREQIRR	$κ_{P, R}^{D I} (T_{g})$ $Mathematical equation: $\kappa_\mathrm{P,R}^\mathrm{DI}(T_\mathrm{g})$$	$κ_{P}^{D I} (T_{⋆})$ $Mathematical equation: $\kappa_\mathrm{P}^\mathrm{DI}(T_\star)$$	$κ_{P, R}^{M 14} (T_{g}, P_{g})$ $Mathematical equation: $\kappa_\mathrm{P,R}^\mathrm{M14}(T_\mathrm{g}, P_\mathrm{g})$$	$κ_{P}^{M 14} (T_{⋆}, P_{g})$ $Mathematical equation: $\kappa_\mathrm{P}^\mathrm{M14}(T_\star, P_\mathrm{g})$$	no
FULL	$κ_{P, R}^{D I} (T_{g})$ $Mathematical equation: $\kappa_\mathrm{P,R}^\mathrm{DI}(T_\mathrm{g})$$	κ^DI(v)	$κ_{P, R}^{M 14} (T_{g}, P_{g})$ $Mathematical equation: $\kappa_\mathrm{P,R}^\mathrm{M14}(T_\mathrm{g}, P_\mathrm{g})$$	κ^M14(v, T_g, P_g)	yes/no

Notes. The superscript DI indicates opacities according to the DIANA standards, while M14 symbolises gas opacities from Malygin et al. (2014).

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